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--- wiki:astronomy:radiative_qauntities [2023/11/14 11:43] – Roy Prouty
+++ wiki:astronomy:radiative_qauntities [2023/11/14 12:25] (current) – removed Roy Prouty
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-The radiative energy of a source can be given either in relative terms via some [[~:..:magnitude|magnitude scale]] or in absolute terms via some measure of [[~:..:radiative_qauntities|radiative quantities]].
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-We know from physics classes that energy is conserved quantity. This makes it a convenient quantity to work with because we can be very clear about defining systems containing sources or sinks that add or remove energy to said system, respectively.\\ \\
-It is impossible to measure all of the radiant energy that an astronomical source radiates. This should be obvious, since we generally only see one size of an astronomical source at a time! Energy ($E$) is measured in units $[E]=Joules,J$((Also of relevance is the cgs units $erg$.  $1 ~erg \equiv 100~ nJ$)).\\ \\
-The total amount of radiant energy an astronomical source radiates away per unit time is called the //luminosity//. Luminosity ($L$) is measured in units of power, $[L]=Watts,W$. Again, it is impossible to measure the luminosity of an astronomical source. We only receive a small fraction of this radiant power. The fraction depends on the area of the detector and the distance between the detector and the astronomical source. \\ \\
-Generally, this detected quantity is called the radiant flux. Radiant flux ($F$) is measured in units of $[F]=W(m^2)^{-1}$. The fraction of the luminosity collected by every square-meter of a detector some distance $r$ away from the center of the source is just the luminosity divided by the surface of a sphere of radius $r$. \\ \\
-$$F=\frac{L}{4\pir^2}$$
-The radiative flux defined thus is the total flux emitted over all wavelengths. This is referred to as the bolometric flux, $F_{bol}$. It is therefore prudent to define the spectral radiative flux ($F_\lambda$) which carries units of $[F_\lambda]=W(m~m^2)^{-1}$.\\ \\
-$$F_{bol} = \int_0^\infty F_\lambda d\lambda = \int_0^\infty F_\nu d\nu$$
-Recall from the discussion on [[~:..:what_the_detector_measures|what detectors measure]] that after calibration of a raw light image to account for the effects of the detector as well as the effects of the atmosphere, the counts that remain associated with each pixel are assumed to be proportional to the amount of radiant energy that fell into the pixel during integration time.
-===== Radiative Energy =====
-The energy associated with the liberation of these electrons is the radiative energy we seek to measure. This energy interacts with the semiconductor substrate and liberates photoelectrons at a rate assumed to be linear with respect to the integration-time.
-$$E = \frac{hc}{\lambda}$$
-Energy carries the normal units Joules ($[E]=~ J$)((Also of relevance is the $erg$.  $1 ~erg \equiv 100~ nJ$)), but be careful! These counts are proportional to the received radiant energy (in the form of photons for this discussion) incident on a //single pixel//. This single pixel receives photons from a specific angular area of the sky, the pixel has an area over which it received photons, an orientation of that area, a time during which it was 'allowed' to receive photons, and a sensitivity to photons over a specific range of wavelengths.\\ \\
-So these counts are proportional not to the total energy of a target observed by the telescope, but to the differential amount of that energy called (in the broadest sense) the spectral radiance.
-===== Spectral Radiance =====
-The differential amount of energy shown in the numerator of the right hand side tends to vanish as the factors in the denominator tend to zero. The spectral radiance (the left hand side; $I(\lambda, \theta, \phi)$) is the limiting value this ratio approaches. Is can be thought of as a "ray" of light or "pencil" of radiation. The spectral radiance is a convenient theoretical quantity since its dependence on differential solid angle leave it conserved over its optical path (barring any sources or sinks). Therefore, the spectral radiance is the basis of all radiative transfer theory.
-$$I(\lambda, \theta, \phi) = \frac{d^6 E}{d\lambda\cdot dt\cdot d^2A \cos{\theta}\cdot d^2\Omega(\theta,\phi)}$$
-The spectral radiance((I have happily glossed over the orientation aspect of the denominator in the above definitions. Strictly speaking, the differential area carries an orientation and the differential solid angle carries with it a unit vector identified by the coordinate pair ($\theta, \phi$). So the differential area and differential solid angle should more appropriately appear first as $d^2\hat{A}\cdot d\hat{\Omega}(\theta, \phi) = d^2A\hat{n}\cdot d\hat{\Omega}(\theta, \phi)$. There the "^" above the symbols speaks to the fact that they are each vector-quantities and the "$\cdot$" this time represents the inner product (dot product in this space). Since there is always a plane of incidence one can rotate the system to without losses, the azimuthal coordinate plays no role and the scalar product that appears above can be directly used: $d^2A\cos{\theta}\cdot d\Omega(\theta,\phi)$. Again, this acts to only integrate the components of the spectral radiances that are parallel to the orientation of the detector, or -- said another way -- impinge the detector perpendicularly.
-{{https://www.researchgate.net/publication/316314426/figure/fig2/AS:566976330334209@1512189099540/Schematic-illustrating-the-geometric-definition-of-spectral-radiance-and-luminance.png?200|}})) has units $[I(\lambda, \theta, \phi)]=J\cdot (m\cdot t\cdot m^2\cdot sr^2)^{-1} = W\cdot (m\cdot m^2\cdot sr^2)^{-1}$\\ \\
-Said slightly differently, the spectral radiance is the amount of energy received by an area ($d^2A$) with some orientation relative to incidence ($\cos{\theta}$) and some a sensitivity to photons over a specific range of wavelengths ($d\lambda$) from a specific angular area of the sky ($d^2\Omega(\theta,\phi)$) during some time ($dt$).\\ \\
-Each pixel effectively integrates this spectral radiance with respect to wavelength, time, perpendicular area, and solid angle. The resulting measure of radiant energy is what is responsible for liberating photoelectrons in the CMOS semiconductor substrate which are eventually readout proportional to a voltage they generate as counts.\\ \\
-===== Spectral Flux =====
-For angularly unresolved sources, we are forced to assume that the energy we received in each pixel is the integral of all the spectral radiance that emerged from the source parallel to our line of sight. Since we only can hope to get components of radiance from one hemisphere of the radiance field generated by the source, we can integrate over half of the sphere ($\theta\in[0,\frac{\pi}{2}], \phi\in[0,2\pi]$).
- $$\int_{2\pi}I(\lambda, \theta, \phi)\cos{\theta}\cdot d^2\Omega(\theta,\phi) = \int_{2\pi}\frac{d^6 E}{d\lambda\cdot dt\cdot d^2A \cos{\theta}\cdot d^2\Omega(\theta,\phi)}\cos{\theta}\cdot d^2\Omega(\theta,\phi)$$
-Note that this is the first angular moment of the spectral radiance field. And it is defined to be the spectral flux.
-$$F(\lambda) = \frac{d^4 E}{d\lambda\cdot dt\cdot d^2A_{\perp}}$$
-The radiative, spectral flux has units $[F(\lambda)]=J\cdot (m\cdot t\cdot m^2)^{-1}=W\cdot (m\cdot m^2)^{-1}$. \\ \\
-BLAH THIS PAGE IS NOT DONE. I need to explain how to photometrically calibrate still with this background out of the way ... maybe this is another page.
-{{tag>[not-done]}}